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arxiv: 2606.11300 · v1 · pith:V6XRDOAHnew · submitted 2026-06-09 · 🌌 astro-ph.CO · astro-ph.IM

Calibration of CMB Polarisation Using Cross-Experiment Correlations

Claire Rigouzzo , Eugene Lim , Susanna Azzoni , Yiqi Liu This is my paper

Pith reviewed 2026-06-27 11:59 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.IM
keywords CMB polarisationcross-correlationspolarisation calibrationcosmic birefringenceSimons ObservatoryPlanck
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The pith

Cross-experiment correlations calibrate CMB polarisation angles to 0.1° without assuming zero birefringence.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper presents a method that determines the relative polarisation misalignment angle between different CMB experiments by analysing their cross-correlations over common sky regions. This data-driven approach avoids the usual assumption that isotropic cosmic birefringence and primordial EB correlations vanish, so it keeps the data sensitive to parity-violating signals. As a concrete demonstration, the authors forecast that a reference calibration of the Simons Observatory small aperture telescopes to 0.08° permits the large aperture telescope to reach 0.10° and Planck to reach 0.17° at roughly 145 GHz. The technique therefore supplies a route to consistent calibration across multiple instruments while still allowing searches for cosmic birefringence and related effects.

Core claim

By solving directly for the relative misalignment angle from cross-experiment correlations, the method achieves the quoted calibration uncertainties for the SO Large Aperture Telescope and Planck while leaving sensitivity to isotropic cosmic birefringence and primordial EB correlations intact.

What carries the argument

Cross-experiment EB correlation analysis that solves for the relative polarisation misalignment angle.

Load-bearing premise

At least one instrument must already be calibrated to the target precision by an independent means such as a wire-grid calibrator, and the cross-correlations must contain enough information to solve for the angle.

What would settle it

If real data from the Simons Observatory and Planck yield calibration uncertainties larger than the forecasted 0.10° and 0.17° when the reference instrument is fixed at 0.08°, the performance claims would not hold.

Figures

Figures reproduced from arXiv: 2606.11300 by Claire Rigouzzo, Eugene Lim, Susanna Azzoni, Yiqi Liu.

Figure 1
Figure 1. Figure 1: Forecast noise power spectra for the SO SATs and [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of the calibration precision σRij be￾tween simulation and analytical result for different frequen￾cies, for both SAT & Planck and SAT & LAT. The frequency channels are 93,145 and 225 GHz for the Simons observatory and 100, 143 and 217 GHz for Planck. For the simulations, we chose ˜α1 = 0.057◦ and ˜α2 = −0.069◦ , and show in a grey dashed line the corresponding fiducial value α1 − α2 = 0.13◦ . Va… view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the standard deviation for the tele [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
read the original abstract

Parity-violating physics in the Universe can generate correlations between the Cosmic Microwave Background (CMB) $E$- and $B$-modes, but detecting such signals requires extremely accurate calibration of instruments. We describe a data-driven method to calibrate the relative polarisation angle between CMB experiments using cross-correlations of observations over a common sky region. Unlike standard self-calibration approaches, this method does not assume vanishing isotropic cosmic birefringence or primordial $EB$ correlations when estimating the relative misalignment angle, and therefore preserves sensitivity to parity-violating physics. As a proof of concept, we forecast the performance of this method using the Simons Observatory (SO) Small Aperture Telescopes (SATs) as a calibrated reference. If they can be calibrated to an uncertainty of $0.08^\circ$, as anticipated from the SO wire grid calibration system, we show that the SO Large Aperture Telescope and Planck could be calibrated to uncertainties of $0.10^\circ$ and $0.17^\circ$, respectively, at $\sim 145$ GHz. This approach relies on the availability of at least one well-calibrated instrument, and provides a complementary path to improving polarisation calibration across experiments, enabling more robust searches for parity-violating physics in the CMB, such as cosmic birefringence.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

0 major / 3 minor

Summary. The manuscript proposes a data-driven method to calibrate the relative polarization angle between CMB experiments via cross-correlations over a common sky region. Unlike self-calibration techniques, the approach does not assume vanishing isotropic cosmic birefringence or primordial EB correlations, thereby preserving sensitivity to parity-violating signals. As a proof of concept, the authors forecast that, given an independent 0.08° calibration uncertainty for the Simons Observatory Small Aperture Telescopes (via wire-grid system), the SO Large Aperture Telescope and Planck can be calibrated to 0.10° and 0.17° respectively at ~145 GHz.

Significance. If the forecasts are borne out, the method supplies a useful complementary calibration route that avoids common assumptions in birefringence searches and can be applied whenever at least one experiment has an independent high-accuracy reference calibration. The quantitative forecasts, conditioned on realistic instrument parameters, constitute a concrete contribution to the field.

minor comments (3)
  1. [Abstract] Abstract: the quoted uncertainties (0.08°, 0.10°, 0.17°) are forecasts resting on modeling choices and simulated data; a brief parenthetical statement of the key assumptions (sky coverage, multipole range, noise model) would improve clarity for readers who do not reach the methods section.
  2. The manuscript would benefit from an explicit statement, perhaps in the introduction or methods, of the functional form used to propagate the reference calibration uncertainty into the cross-experiment constraints (e.g., via a Fisher matrix or Monte-Carlo pipeline).
  3. Consider adding a short table that tabulates the forecasted angle uncertainties for each experiment pair together with the assumed reference uncertainty and the effective sky overlap fraction.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of the manuscript, including the recognition of its significance as a complementary calibration approach that avoids assumptions about birefringence or primordial EB. We appreciate the recommendation for minor revision. No specific major comments were provided in the report.

Circularity Check

0 steps flagged

No significant circularity

full rationale

The paper's central result is an explicit conditional forecast: given independent wire-grid calibration of SO SATs to 0.08°, cross-correlations over common sky are forecasted to yield 0.10° (SO LAT) and 0.17° (Planck) at ~145 GHz. The abstract states the reference requirement and the avoidance of EB=0 or isotropic birefringence assumptions. No equation reduces the output uncertainties to quantities fitted from the same data being calibrated, no self-citation chain is load-bearing for the forecast, and the method is presented as complementary to external calibration rather than self-contained. The derivation therefore remains self-contained against the stated external benchmark.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The forecast depends on an external calibration accuracy for the reference instrument and on the assumption that cross-power spectra between experiments contain usable information about relative angle. No new physical entities are introduced.

free parameters (1)
  • reference calibration uncertainty
    0.08° for SO SATs is taken as given from the wire-grid system; the derived uncertainties for other instruments scale directly from this input value.
axioms (1)
  • domain assumption Cross-correlations over common sky region encode the relative polarization misalignment angle independently of isotropic birefringence or primordial EB signals.
    This is the central modeling premise that allows the method to avoid the assumptions it criticizes in self-calibration.

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